Universe in a box:simulating formation of cosmic structures

Andrey KravtsovDepartment of Astronomy & AstrophysicsCenter for Cosmological Physics (CfCP)

University of Chicago

http://astro.uchicago.edu/~andrey/talks/http://cfcp.uchicago.edu/lss/

Galaxies

Galaxy Clusters

Supergalactic plane on the sky

Branchini et al. 1998

The LocalSupercluster

Gerard de Vaucouleurs 1918-1995 on the sky

Large-scale structure of the Universe

as seenby the

CfA survey

On even larger scales... (billions of light years)

Structures in the Universe

graphics from Wayne Hu (background.uchicago.edu/~whu)

Formation of structuresas cosmologists envision it

Big Bang

z=1066

First particlesform

Light elements(H, He, Li)

formz=100000

Universe becomesneutral

z=1000

Galaxies form

z~1-5

First stars formUniverse is reionized

z~10

Solar systemformsz~0.4

Present day

z=0

Content of the Universe: all existing components

(protons, neutrons, hypothetical dark matter)

contribute to gravity and can influence the rate with which

the Universe expandsó The contribution of each component is measured in units of critical density: Ωi = ρ/ ρcrit

Content of the Universe: observational probes

% Cosmic Microwave Background ripplesõ physics causing 10-5 deviations from the uniform black body

temperature is very well understood in a given model. Observablestatistics of fluctuations (e.g., angular correlation function or power spectrum) depend on cosmological parameters, including matter and energy content.

% Large-scale structure of the Universeí galaxies, galaxy clusters, filaments

% Standard "candles"ð any object whose intrinsic brightness is known or can be deduced

from observations without using distance. SNIa are currently the best cosmological standard candles known

% Standard rulers (systems with known intrinsic size)

Cosmic Microwave Background (CMB) Temperature Anisotropies

Wilkinson Microwave Anistropy Probe (WMAP) satellite resultscirca February 2003

High redshift supernovae type Ia

SNAP satellite proposal

Cosmic Pie

Computer Simulations: How to set up and where to

begin? % If the content of the Universe is assumed, theory predicts the statistical properties of inhomogeneities in matter distribution

õ these predictions are used to set up initial conditions of the simulations

% Simple analytic predictions are accurate only while inhomogeneities are small (<10% fluctuations with respect to the mean density of the Universe)

í simulations are initialized at an epoch before analytic predictions break down, during the so-called "Dark Ages"

% Numerical simulations are used to follow formation of structures and make accurate predictions at later epochs where analytic calculations break down

ð

Computer Simulations: How do we model?

% Gravity is the kingõ gravity is by far the strongest force on

the large scales. gravitational interactions are modelled using Newton's laws

% Other forces may need to be included depending on the composition of the Universe and scales considered

í ordinary matter, the baryons, experiences pressure forces if compressed to sufficiently high densities. these "hydrodynamic" forces are included in simulations that include baryons

We all live in

Cosmological Redshift as a measure of distance

and time

redshift

Distance

Age of the

Universe

Computer Simulations: discretizing matter and space

% Space and time are continuous on macroscopic scales, but computers can only deal with discrete numbers

% Memory and CPU speed limit the number of volume elements and particles that we can simulate

í in the standard theories, 1051-1082 dark matter particles are expected in a cubic Megaparsec

í current computers can handle only up to a billion particles

í ----> need to discretize

HardwareSupercomputers at National Centers and Labs

(e.g., the National Center for Supercomputer Applications -NCSA)

www.ncsa.uiuc.edu

Lots and lots of storage...

Many Many Lines of Software

Universe in a Box:modelling formation of

structures redshift = 10; 13 billion years ago

Universe in a Box:modelling formation of

structures redshift = 5; 12.3 billion years ago

Universe in a Box:modelling formation of

structures redshift = 3; 11.4 billion years ago

Universe in a Box:modelling formation of

structures redshift = 1; 7.7 billion years ago

Universe in a Box:modelling formation of

structures redshift = 0; today

43 Mpc ΛCDM

4 Mpc ΛCDM

Baryons: sloshing, shocking, cooling

From darkness to light:the messy physics of galactic

kitchen

To model formation of galaxieswe need to deal with "gastrophysics"...

Towards simulating realistic galaxies